Papers › The structure and assembly history of cluster-size haloes in Self-Interacting Dark Matter
The structure and assembly history of cluster-size haloes in Self-Interacting Dark Matter
Thejs Brinckmann, Jesús Zavala, David Rapetti, Steen H. Hansen, Mark Vogelsberger
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We perform dark-matter-only simulations of 28 relaxed massive cluster-sized haloes for Cold Dark Matter (CDM) and Self-Interacting Dark Matter (SIDM) models, to study structural differences between the models at large radii, where the impact of baryonic physics is expected to be very limited. We find that the distributions for the radial profiles of the density, ellipsoidal axis ratios, and velocity anisotropies (β) of the haloes differ considerably between the models (at the ∼1σ level), even at ≳10% of the virial radius, if the self-scattering cross section is σ/mᵪ=1 cm² gr⁻¹. Direct comparison with observationally inferred density profiles disfavours SIDM for σ/mᵪ=1 cm² gr⁻¹, but in an intermediate radial range (∼3% of the virial radius), where the impact of baryonic physics is uncertain. At this level of the cross section, we find a narrower β distribution in SIDM, clearly skewed towards isotropic orbits, with no SIDM (90% of CDM) haloes having β>0.12 at 7% of the virial radius. We estimate that with an observational sample of ∼30 (∼10¹⁵ M_⊙) relaxed clusters, β can potentially be used to put competitive constraints on SIDM, once observational uncertainties improve by a factor of a few. We study the suppression of the memory of halo assembly history in SIDM clusters. For σ/mᵪ=1 cm² gr⁻¹, we find that this happens only in the central halo regions (∼1/4 of the scale radius of the halo), and only for haloes that assembled their mass within this region earlier than a formation redshift z_f∼2. Otherwise, the memory of assembly remains and is reflected in ways similar to CDM, albeit with weaker trends.
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